Search the World Wide Web for information about the latest observations of the stellar remnant at the center of SN \(1987 \mathrm{~A}\). Has a pulsar been detected? If so, how fast is it spinning? Has the supernova's debris thinned out enough to give a clear view of the neutron star?

In the cosmic aftermath of a supernova explosion, the core of the once mighty star often becomes what is known as a 'stellar remnant.' These remnants can take the form of white dwarfs, neutron stars, or black holes, depending on the original mass of the star.

Neutron stars are particularly interesting stellar remnants due to their incredibly dense nature. They are about as massive as the sun but have a radius of only about 10 kilometers. Imagine squeezing a mass over one million times that of the Earth into a ball no larger than a small city – this is the case with neutron stars. They possess strong magnetic fields and as they rotate, emit beams of electromagnetic radiation observable as pulses when the beam's path crosses the Earth, hence being termed 'pulsars.'

When a star like the one in SN1987A explodes, the core collapses so rapidly that protons and electrons combine to form neutrons. Such a sudden collapse and subsequent 'bounce' back qualitatively explains the massive explosion seen in supernovae, leaving behind a neutron star at its heart.

Detecting a pulsar involves capturing the tell-tale pulses of radiation that neutron stars emit. Astronomers use radio telescopes to scan the skies for these signals, which can be identified by their distinctive, highly regular pattern. The recent searches around the site of SN1987A aim to spot such periodic signals, which would confirm the presence of a pulsar.

When a pulsar is detected, astronomers can measure the interval between pulses to determine the rotation speed of the neutron star. These rotation speeds can be astonishing, with some pulsars spinning hundreds of times per second. Discovering a pulsar can significantly advance our understanding of the life cycle of stars and the nature of supernovae.

The visibility of a neutron star after a supernova explosion depends significantly on the distribution and density of the debris, or 'supernova remnant,' surrounding it. Initially, this debris is thick and opaque, obscuring our view of the collapsed star's core.

However, as time progresses, this material slowly disperses. If the supernova's debris thins out sufficiently, astronomers can potentially get a clear view of the neutron star. This process might take years or decades. As the debris clears, not only does the neutron star become visible, but detailed observations can lead to valuable data on the properties and behaviors of such exotic objects.

The remnants of a supernova are composed of the outer layers of the original star, scattered across space in a violent explosion. This debris is rich with heavy elements forged in the stellar furnace and dispersed by the supernova event, seeding future generations of stars and planets with the materials necessary for life.

The debris cloud expands over time, becoming less dense. As it does so, it can reveal the cosmic treasures hidden within its core—like a neutron star. Observations of this dispersing material not only help in understanding the explosion mechanics and the progenitor star's life but also in unveiling potential hidden celestial objects like pulsars. The study of this debris is crucial for piecing together the vast puzzle of stellar evolution and the chemical enrichment of the universe.